TOI-858 B b: A hot Jupiter on a polar orbit in a loose binary

Hagelberg, J.; Nielsen, L. D.; Attia, M.; Bourrier, V.; Pearce, L.; Venturini, J.; Winn, J. N.; Bouchy, F.; Bouma, L. G.; Briceño, C.; Collins, K. A.; Davis, A. B.; Eastman, J. D.; Evans, P.; Falk, B.; Grieves, N.; Guerrero, N. M.; Hellier, C.; Jones, M. I.; Latham, D. W.; Law, N.; Mann, A. W.; Marmier, M.; Ottoni, G.; Radford, D. J.; Restori, N.; Rudat, A.; Dos Santos, L.; Seager, S.; Stassun, K.; Stockdale, C.; Udry, S.; Wang, S.; Ziegler, C.

doi:10.1051/0004-6361/202244940

A&A

2023

DOI: 10.1051/0004-6361/202244940

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TOI-858 B b: A hot Jupiter on a polar orbit in a loose binary

J. Hagelberg,

L. D. Nielsen,

M. Attia

et al.

Abstract: We report the discovery of a hot Jupiter on a 3.28-day orbit around a 1.08 M⊙ G0 star that is the secondary component in a loose binary system. Based on follow-up radial velocity observations of TOI-858 B with CORALIE on the Swiss 1.2 m telescope and CHIRON on the 1.5 m telescope at the Cerro Tololo Inter-American Observatory (CTIO), we measured the planet mass to be 1.10−0.07+0.08 MJ. Two transits were further observed with CORALIE to determine the alignment of TOI-858 B b with respect to its host star. Analy… Show more

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2024

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Cited by 3 publications

References 107 publications

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Obliquities of exoplanet host stars

Knudstrup,

Albrecht,

Winn

et al. 2024

A&A

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Measurements of the obliquities in exoplanet systems have revealed some remarkable architectures, some of which are very different from the Solar System. Nearly 200 obliquity measurements have been obtained through observations of the Rossiter–McLaughlin (RM) effect. Here, we report on observations of 19 planetary systems that led to 17 clear detections of the RM effect and 2 less secure detections. After adding the new measurements to the tally, we used the entire collection of RM measurements to investigate four issues that have arisen in the literature. i) Does the obliquity distribution show a peak at approximately 90°? We find tentative evidence that such a peak does exist when restricting attention to the sample of sub-Saturn planets and hot Jupiters orbiting F stars. ii) Are high obliquities associated with high eccentricities? We find the association to be weaker than previously reported, and that a stronger association exists between obliquity and orbital separation, possibly due to tidal obliquity damping at small separations. iii) How low are the lowest known obliquities? Among hot Jupiters around cool stars, we find the dispersion to be 1.4 ± 0.7°, smaller than the 6° obliquity of the Sun, which serves as additional evidence for tidal damping. iv) What are the obliquities of stars with compact and flat systems of multiple planets? We find that they generally have obliquities lower than 10°, with several remarkable exceptions possibly caused by wide-orbiting stellar or planetary companions.

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Obliquities of exoplanet host stars

Knudstrup,

Albrecht,

Winn

et al. 2024

A&A

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Viewing the PLATO LOPS2 field through the lenses of TESS

Eschen,

Bayliss,

Wilson

et al. 2024

Monthly Notices of the Royal Astronomical Society

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PLATO will begin observing stars in its Southern Field (LOPS2) after its launch in late 2026. By this time, TESS will have observed the stars in LOPS2 for at least four years. We find that by 2025, on average each star in the PLATO field will have been monitored for 330 days by TESS, with a subset of stars in the TESS continuous viewing zone having over 1000 days of monitoring. There are currently 101 known transiting exoplanets in the LOPS2 field, with 36 of these residing in multiplanet systems. The LOPS2 field also contains more than 500 TESS planet candidate systems, 64 exoplanets discovered by radial velocity only, over 1000 bright (V<13) eclipsing binary systems, 7 transiting brown dwarf systems, and 2 bright white dwarfs (G<13). We calculate TESS and PLATO sensitivities to detecting transits for the bright FGK stars that make up the PLATO LOPS2 P1 sample. We find that TESS should have discovered almost all transiting giant planets out to approximately 30 d within the LOPS2 field, and out to approximately 100 d for the regions of the LOPS2 field within the TESS CVZ (∼20 per cent of the LOPS2 field). However, we find that for smaller radius planets in the range 1 – 4 R⊕ PLATO will have significantly better sensitivity, and these are likely to make up the bulk of new PLATO discoveries.

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On the origin of polar planets around single stars

Chen,

Baronett,

Nixon

et al. 2024

Monthly Notices of the Royal Astronomical Society: Letters

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The Rossiter–McLaughlin effect measures the misalignment between a planet’s orbital plane and its host star’s rotation plane. Around 10 per cent of planets exhibit misalignments in the approximate range 80°–125°, with their origin remaining a mystery. On the other hand, large misalignments may be common in eccentric circumbinary systems due to misaligned discs undergoing polar alignment. If the binary subsequently merges, a polar circumbinary disc – along with any planets that form within it – may remain inclined near 90$^{\circ }$ to the merged star’s rotation. To test this hypothesis, we present N-body simulations of the evolution of a polar circumbinary debris disc comprised of test particles around an eccentric binary during a binary merger that is induced by tidal dissipation. After the merger, the disc particles remain on near-polar orbits. Interaction of the binary with the polar-aligned gas disc may be required to bring the binary to the small separations that trigger the merger by tides. Our findings imply that planets forming in discs that are polar-aligned to the orbit of a high-eccentricity binary may, following the merger of the binary, provide a possible origin for the population of near-polar planets around single stars.

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TOI-858 B b: A hot Jupiter on a polar orbit in a loose binary

Cited by 3 publications

References 107 publications

Obliquities of exoplanet host stars

Obliquities of exoplanet host stars

Viewing the PLATO LOPS2 field through the lenses of TESS

On the origin of polar planets around single stars

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